Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004pasj...56..181f&link_type=abstract
Publications of the Astronomical Society of Japan, Vol.56, No.1, pp. 181-192
Astronomy and Astrophysics
Astronomy
7
Accretion, Accretion Disks, Astrophysical Jets, Galaxies: Active, Stars: Winds, Outflows, X-Rays: Stars
Scientific paper
We examine a hydrodynamical wind, which emanates from an accretion disk and is driven by thermal, magnetic, and radiation pressures, under a one-dimensional approximation along supposed streamlines. The disk gas is assumed to be isothermal, the magnetic field has only a toroidal component, and the radiation field is evaluated along the streamline. Such a disk wind is characterized by an isothermal sound speed, the Alfvén speed at the footpoint, and the strength of radiation fields. Isothermal winds can always blow even in the cold less-luminous case, and transonic winds are established, except for the perfectly cold case without thermal pressure. Beyond some critical luminosity, disk winds are always supersonic, irrespective of the thermal and magnetic pressures. We found that the terminal speed v∞ is roughly expressed as (1/2) v∞2 = (1/2) v02 - (1/2) (GM/r0) + 10.5 aT2 + 0.7 aAO2 + 16 Γeff (GM/r0), where v0 is the initial velocity, M the mass of the central object, r0 the radius of the wind base on the disk, aT the isothermal sound speed, aA0 the initial Alfvén speed, and Γeff the effective normalized luminosity, although the coefficients depend on the configuration of the streamlines.
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